论文标题
在积聚中子星中热释放
Heat release in accreting neutron stars
论文作者
论文摘要
据信，观察到来自静态状态下的中子星（NSS）的热发射，被认为是由加热恒星外壳（深层地壳加热范式）的非平衡核反应提供动力的。假设NS具有完全积聚的外壳，我们为加热效率提供了一个简单的通用公式。我们进一步表明，在最近提出的热力学一致的方法中，可以通过唯一的一个参数来参数释放 - 压力$ p _ {\ rm oi} $在外部壳界面处的压力$ p _ {\ rm oi} $（正如我们所说的那样，这种压力不一定应与中子滴定压力重合）。我们讨论了$ p _ {\ rm oi} $的可能值，以选择解释外壳效果的核模型，并确定净热量释放及其在地壳中的分布，这是$ p _ {\ rm oi} $的函数。我们得出的结论是，与以前的作品相比，将热量释放量应减少几乎不到。
Observed thermal emission from accreting neutron stars (NSs) in a quiescent state is believed to be powered by nonequilibrium nuclear reactions that heat the stellar crust (deep crustal heating paradigm). We derive a simple universal formula for the heating efficiency, assuming that an NS has a fully accreted crust. We further show that, within the recently proposed thermodynamically consistent approach to the accreted crust, the heat release can be parametrized by the only one parameter -- the pressure $P_{\rm oi}$ at the outer-inner crust interface (as we argue, this pressure should not necessarily coincide with the neutron-drip pressure). We discuss possible values of $P_{\rm oi}$ for a selection of nuclear models that account for shell effects, and determine the net heat release and its distribution in the crust as a function of $P_{\rm oi}$. We conclude that the heat release should be reduced by a factor of few in comparison to previous works.
